AAS Worldwide Telescope: Seamless, Cross-Platform Data Visualization Engine for Astronomy Research, Education, and Democratizing Data
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XAMARIN.FORMS for BEGINNERS ABOUT ME Tom Soderling Sr
XAMARIN.FORMS FOR BEGINNERS ABOUT ME Tom Soderling Sr. Mobile Apps Developer @ Polaris Industries; Ride Command Xamarin.Forms enthusiast DevOps hobbyist & machine learning beginner 4 year XCMD Blog: https://tomsoderling.github.io GitHub: https://github.com/TomSoderling Twitter: @tomsoderling How Deep Pickster Spaniel Is It? THE PLAN • Introduction: Why, What, and When • Overview of Xamarin.Forms Building Blocks • Building a Xamarin.Forms UI in XAML • Data Binding • View Customization • Next Steps & Resources • Please ask any questions that come up! THE PLAN • Introduction: Why, What, and When • Overview of Xamarin.Forms Building Blocks • Building a Xamarin.Forms UI in XAML • Data Binding • View Customization • Next Steps & Resources INTRODUCTION : WHY • WET: the soggy state of mobile app development • Write Everything Twice INTRODUCTION : WHY • WET: the soggy state of mobile app development • Write Everything Twice INTRODUCTION : WHAT • What is Xamarin.Forms? • Cross-platform UI framework • Platforms: • Mobile: iOS 8 and up, Android 4.0.3 (API 15) • Desktop: Windows 10 UWP, MacOS, WFP • Samsung Smart Devices: Tizen INTRODUCTION : WHAT • Brief History: • May 2011, Xamarin founded • MonoTouch and Mono for Android using MonoDevelop IDE • February 2013, release of Xamarin 2.0 • Xamarin Studio IDE & integration with Visual Studio • Renamed to Xamarin.Android and Xamarin.iOS • May 2014, Xamarin.Forms released as part of Xamarin 3 • February 24 2016, Xamarin acquired by Microsoft • Owned, actively developed on, and supported by Microsoft • Free -
Space Astronomy in the 90S
Space Astronomy in the 90s Jonathan McDowell April 26, 1995 1 Why Space Astronomy? • SHARPER PICTURES (Spatial Resolution) The Earth’s atmosphere messes up the light coming in (stars twinkle, etc). • TECHNICOLOR (X-ray, infrared, etc) The atmosphere also absorbs light of different wavelengths (col- ors) outside the visible range. X-ray astronomy is impossible from the Earth’s surface. 2 What are the differences between satellite instruments? • Focussing optics or bare detectors • Wavelength or energy range - IR, UV, etc. Different technology used for different wavebands. • Spatial Resolution (how sharp a picture?) • Spatial Field of View (how large a piece of sky?) • Spectral Resolution (can it tell photons of different energies apart?) • Spectral Field of View (bandwidth) • Sensitivity • Pointing Accuracy • Lifetime • Orbit (hence operating efficiency, background, etc.) • Scan or Point What are the differences between satellites? • Spinning or 3-axis pointing (older satellites spun around a fixed axis, precession let them eventually see different parts of the sky) • Fixed or movable solar arrays (fixed arrays mean the spacecraft has to point near the plane perpendicular to the solar-satellite vector) 3 • Low or high orbit (low orbit has higher radiation, atmospheric drag, and more Earth occultation; high orbit has slower preces- sion and no refurbishment opportunity) • Propulsion to raise orbit? • Other consumables (proportional counter gas, attitude control gas, liquid helium coolant) 4 What are the differences in operation? • PI mission vs. GO mission PI = Principal Investigator. One of the people responsible for building the satellite. Nowadays often referred to as IPIs (In- strument PIs). GO = Guest Observer. Someone who just want to use the satel- lite. -
Licensing Information User Manual Release 9.1 F13415-01
Oracle® Hospitality Cruise Fleet Management Licensing Information User Manual Release 9.1 F13415-01 August 2019 LICENSING INFORMATION USER MANUAL Oracle® Hospitality Fleet Management Licensing Information User Manual Version 9.1 Copyright © 2004, 2019, Oracle and/or its affiliates. All rights reserved. This software and related documentation are provided under a license agreement containing restrictions on use and disclosure and are protected by intellectual property laws. Except as expressly permitted in your license agreement or allowed by law, you may not use, copy, reproduce, translate, broadcast, modify, license, transmit, distribute, exhibit, perform, publish, or display any part, in any form, or by any means. Reverse engineering, disassembly, or decompilation of this software, unless required by law for interoperability, is prohibited. The information contained herein is subject to change without notice and is not warranted to be error- free. If you find any errors, please report them to us in writing. If this software or related documentation is delivered to the U.S. Government or anyone licensing it on behalf of the U.S. Government, then the following notice is applicable: U.S. GOVERNMENT END USERS: Oracle programs, including any operating system, integrated software, any programs installed on the hardware, and/or documentation, delivered to U.S. Government end users are "commercial computer software" pursuant to the applicable Federal Acquisition Regulation and agency-specific supplemental regulations. As such, use, duplication, disclosure, modification, and adaptation of the programs, including any operating system, integrated software, any programs installed on the hardware, and/or documentation, shall be subject to license terms and license restrictions applicable to the programs. -
Particle Acceleration in Solar Flares What Is the Link Between Heating and Particle Acceleration?
Energetic Particles in the Solar Atmosphere (X- ray diagnostics) Nicole Vilmer LESIA, Observatoire de Paris, CNRS, UPMC, Université Paris-Diderot The Sun as a Particle Accelerator: First detection of energetic protons from the Sun(1942) (related to a solar flare) First X-ray observations of solar flares (1970) Chupp et al., 1974 First observations of -ray lines from solar flares (OSO7/Prognoz 1972) Since then many more observations With e.g. RHESSI (2002-2018) And also INTEGRAL, FERMI >120000 X-ray flares observed by RHESSI (NASA/SMEX; 2002-2018) But still a limited number of gamma- ray line flares ~30 Solar flare: Sudden release of magnetic energy Heating Particle acceleration X-rays 6-8 keV 25-80 keV 195 Å 304 Å 21 aug 2002 (extreme ultraviolet) 335 Å 15 fev 2011 HXR/GR diagnostics of energetic electrons and ions SXR emission Hot Plasma (7to 8 MK ) HXR emission Bremsstrahlung from non-thermal electrons Prompt -ray lines : Deexcitation lines(C and 0) (60%) Signature of energetic ions (>2 MeV/nuc) Neutron capture line: p –p ; p-α and p-ions interactions Production of neutrons Collisional slowing down of neutrons Radiative capture on ambient H deuterium + 2.2 MeV. line RHESSI Observations X/ spectrum Thermal components T= 2 10 7 K T= 4 10 7 K Electron bremsstrahlung Ultrarelativistic -ray lines Electron (ions > 3 MeV/nuc) Bremsstrahlung (INTEGRAL) SMM/GRS PHEBUS/GRANAT FERMI/LAT observations RHESSI Pion decay radiation(ions > ~300MeV/nuc) Particle acceleration in solar flares What is the link between heating and particle acceleration? Where are the acceleration sites? What is the transport of particles from acceleration sites to X/ γ ray emission sites? What are the characteristic acceleration times? RHESSI How many energetic particles? Energy spectra? Relative abundances of energetic ions? RHESSI Which acceleration mechanisms in solar flares? Shock acceleration? Stochastic acceleration? (wave-particle interaction) Direct Electric field acceleration. -
Seeing the Sky Visualization & Astronomers
Seeing the Sky Visualization & Astronomers Alyssa A. Goodman Harvard Smithsonian Center for Astrophysics & Radcliffe Institute for Advanced Study @aagie WorldWide Telescope Gm1m2 F= gluemultidimensional data exploration R2 Cognition “Paper of the Future” Language* Data Pictures Communication *“Language” includes words & math Why Galileo is my Hero Explore-Explain-Explore Notes for & re-productions of Siderius Nuncius 1610 WorldWide Telescope Galileo’s New Order, A WorldWide Telescope Tour by Goodman, Wong & Udomprasert 2010 WWT Software Wong (inventor, MS Research), Fay (architect, MS Reseearch), et al., now open source, hosted by AAS, Phil Rosenfield, Director see wwtambassadors.org for more on WWT Outreach WorldWide Telescope Galileo’s New Order, A WorldWide Telescope Tour by Goodman, Wong & Udomprasert 2010 WWT Software Wong (inventor, MS Research), Fay (architect, MS Reseearch), et al., now open source, hosted by AAS, Phil Rosenfield, Director see wwtambassadors.org for more on WWT Outreach Cognition “Paper of the Future” Language* Data Pictures Communication *“Language” includes words & math enabled by d3.js (javascript) outputs d3po Cognition Communication [demo] [video] Many thanks to Alberto Pepe, Josh Peek, Chris Beaumont, Tom Robitaille, Adrian Price-Whelan, Elizabeth Newton, Michelle Borkin & Matteo Cantiello for making this posible. 1610 4 Centuries from Galileo to Galileo 1665 1895 2009 2015 WorldWide Telescope Gm1m2 F= gluemultidimensional data exploration R2 WorldWide Telescope gluemultidimensional data exploration WorldWide Telescope gluemultidimensional data exploration Data, Dimensions, Display 1D: Columns = “Spectra”, “SEDs” or “Time Series” 2D: Faces or Slices = “Images” 3D: Volumes = “3D Renderings”, “2D Movies” 4D:4D Time Series of Volumes = “3D Movies” Data, Dimensions, Display Spectral Line Observations Loss of 1 dimension Mountain Range No loss of information Data, Dimensions, Display mm peak (Enoch et al. -
Software License Agreement (EULA)
Third-party Computer Software AutoVu™ ALPR cameras • angular-animate (https://docs.angularjs.org/api/ngAnimate) licensed under the terms of the MIT License (https://github.com/angular/angular.js/blob/master/LICENSE). © 2010-2016 Google, Inc. http://angularjs.org • angular-base64 (https://github.com/ninjatronic/angular-base64) licensed under the terms of the MIT License (https://github.com/ninjatronic/angular-base64/blob/master/LICENSE). © 2010 Nick Galbreath © 2013 Pete Martin • angular-translate (https://github.com/angular-translate/angular-translate) licensed under the terms of the MIT License (https://github.com/angular-translate/angular-translate/blob/master/LICENSE). © 2014 [email protected] • angular-translate-handler-log (https://github.com/angular-translate/bower-angular-translate-handler-log) licensed under the terms of the MIT License (https://github.com/angular-translate/angular-translate/blob/master/LICENSE). © 2014 [email protected] • angular-translate-loader-static-files (https://github.com/angular-translate/bower-angular-translate-loader-static-files) licensed under the terms of the MIT License (https://github.com/angular-translate/angular-translate/blob/master/LICENSE). © 2014 [email protected] • Angular Google Maps (http://angular-ui.github.io/angular-google-maps/#!/) licensed under the terms of the MIT License (https://opensource.org/licenses/MIT). © 2013-2016 angular-google-maps • AngularJS (http://angularjs.org/) licensed under the terms of the MIT License (https://github.com/angular/angular.js/blob/master/LICENSE). © 2010-2016 Google, Inc. http://angularjs.org • AngularUI Bootstrap (http://angular-ui.github.io/bootstrap/) licensed under the terms of the MIT License (https://github.com/angular- ui/bootstrap/blob/master/LICENSE). -
A New Polarimeter to Study the Curl Component of the Cosmic Microwave Background Polarization
UNIVERSITA` DEGLI STUDI DI ROMA \LA SAPIENZA" Facolt`adi Scienze Matematiche Fisiche e Naturali A new polarimeter to study the curl component of the Cosmic Microwave Background polarization Tesi di Laurea Specialistica in Astronomia ed Astro¯sica Anno Accademico 2005/2006 Author Supervisor Lorenzo Moncelsi Prof. Paolo de Bernardis Register: 1071681 Co-supervisor Dott. Federico Nati Contents Introduzione 6 Introduction 10 1 The Hot Big Bang Model and the Inflation add-on 11 1.1 Introduction . 11 1.2 The Standard Cosmological Model . 11 1.3 The Unsolved Problems . 17 1.3.1 The flatness problem . 17 1.3.2 The horizons problem . 18 1.3.3 The absence of magnetic monopoles . 19 1.4 The Solution: Inflation . 20 1.5 The Physics of Inflation . 22 1.5.1 Scalar Fields . 22 1.5.2 Slow-Roll Approximation . 25 1.5.3 Exact Solutions . 26 1.5.4 Hamilton-Jacobi Formulation . 28 1.5.5 Reheating . 29 1.5.6 Scalar Fluctuations . 30 1.5.7 Tensor Fluctuations . 34 2 The Cosmic Microwave Background 37 2.1 Introduction . 37 2.2 Earth's Absolute Motion: The Dipole Anisotropy . 39 2.3 The Last Scattering Surface . 42 2.4 The Temperature Power Spectrum . 44 2.4.1 Physical E®ects at Recombination . 44 2.4.2 Statistical Treatment . 47 2.4.3 The Shape of the Spectrum . 49 2.5 Polarization . 54 2.5.1 Thomson Scattering at Recombination . 54 2.5.2 Statistical Treatment . 56 2.5.3 Quadrupole Anisotropy From Scalar Perturbations . 65 I 2.5.4 Quadrupole Anisotropy From Tensor Perturbations . -
How Github Secures Open Source Software
How GitHub secures open source software Learn how GitHub works to protect you as you use, contribute to, and build on open source. HOW GITHUB SECURES OPEN SOURCE SOFTWARE PAGE — 1 That’s why we’ve built tools and processes that allow GitHub’s role in securing organizations and open source maintainers to code securely throughout the entire software development open source software lifecycle. Taking security and shifting it to the left allows organizations and projects to prevent errors and failures Open source software is everywhere, before a security incident happens. powering the languages, frameworks, and GitHub works hard to secure our community and applications your team uses every day. the open source software you use, build on, and contribute to. Through features, services, and security A study conducted by the Synopsys Center for Open initiatives, we provide the millions of open source Source Research and Innovation found that enterprise projects on GitHub—and the businesses that rely on software is now comprised of more than 90 percent them—with best practices to learn and leverage across open source code—and businesses are taking notice. their workflows. The State of Enterprise Open Source study by Red Hat confirmed that “95 percent of respondents say open source is strategically important” for organizations. Making code widely available has changed how Making open source software is built, with more reuse of code and complex more secure dependencies—but not without introducing security and compliance concerns. Open source projects, like all software, can have vulnerabilities. They can even be GitHub Advisory Database, vulnerable the target of malicious actors who may try to use open dependency alerts, and Dependabot source code to introduce vulnerabilities downstream, attacking the software supply chain. -
Centaurus a at Hard X-Rays and Gamma Rays
Centaurus A at Hard X-Rays and Soft Gamma-Rays Chandra 1-10 keV CGRO-COMPTEL 1 ± 30 MeV Fermi 100 MeV ± 100 GeV Helmut Steinle Max-Planck-Institut für extraterrestrische Physik Garching, Germany ----------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------- The Many Faces of Centaurus A ± Sydney, 28 June ± 3 July 2009; H. Steinle, MPE 1 / 35 Centaurus A at Hard X-Rays and Soft Gamma-Rays Contents · Introduction · The Spectral Energy Distribution · Properties of the existing measurements in the hard X-ray / soft Gamma-ray regime · Important satellites for this energy / frequency range · Variability of the X-ray / Gamma-ray emission · Two examples of models for the Cen A Spectral Energy Distribution · Problems (features) to be considered when using the hard X-ray / soft Gamma-ray data ± the ªsoft X-ray transient problemº ± the ªSED problemº · Outlook ----------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------- The Many Faces of Centaurus A ± Sydney, 28 June ± 3 July 2009; H. Steinle, MPE 2 / 35 Centaurus A at Hard X-Rays and Soft Gamma-Rays ------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------------- Introduction In the introductory (ªsetting the stageº) section of the -
Experiments on the Differential Vlbi Measurements with the Former Russian Deep Space Network
EXPERIMENTS ON THE DIFFERENTIAL VLBI MEASUREMENTS WITH THE FORMER RUSSIAN DEEP SPACE NETWORK Igor E. Molotov(1,2,3) (1)Bear Lakes Radio Astronomy Station of Central (Pulkovo) Astronomical Observatory, Pulkovskoye chosse 65/1, Saint-Petersburg, 196140, Russia , E-mail: [email protected] (2)Keldysh Institute of Applied Mathematics, Miusskaja sq. 4, 125047 Moscow, Russia (3)Central Research Institute for Machine Building, 4 Pionerskaya Street, Korolev, 141070, Russia ABSTRACT The differential VLBI technique (delta-VLBI) is applied transforms the signals into video frequencies, which for measuring spacecraft position with accuracy up to 1 then are sampled with 1- or 2-bit quantization, formatted in any standard VLBI format (Mk-4, S2, K-4, mas. This procedure allows to link the sky position of object with the position of close ICRF quasar on the Mk-2) and recorded on magnetic tapes or PC-disks celestial sphere. Few delta-VLBI measurements can together with precise clock using VLBI terminal. All frequency transformations are connected with atomic urgently improve the knowledge of object trajectory in the times of critical maneuvers. frequency standard. The tapes/disks from all radio telescopes of VLBI array are collected at data The Russian Deep Space Network that was based on processing center, where the data are cross-correlated. three large antennas: 70 m in Evpatoria (Ukraine) and The processing is aimed to measure the time delay of Ussuriysk (Far East), and 64 m in Bear Lakes (near emitted wavefront arrival to receiving antennas, and Moscow) arranged the trial delta-VLBI experiments frequency of interference (fringe rate), that contain the with help of four scientific institutions. -
GRANAT/WATCH Catalogue of Cosmic Gamma-Ray Bursts: December 1989 to September 1994? S.Y
ASTRONOMY & ASTROPHYSICS APRIL I 1998,PAGE1 SUPPLEMENT SERIES Astron. Astrophys. Suppl. Ser. 129, 1-8 (1998) GRANAT/WATCH catalogue of cosmic gamma-ray bursts: December 1989 to September 1994? S.Y. Sazonov1,2, R.A. Sunyaev1,2, O.V. Terekhov1,N.Lund3, S. Brandt4, and A.J. Castro-Tirado5 1 Space Research Institute, Russian Academy of Sciences, Profsoyuznaya 84/32, 117810 Moscow, Russia 2 Max-Planck-Institut f¨ur Astrophysik, Karl-Schwarzschildstr 1, 85740 Garching, Germany 3 Danish Space Research Institute, Juliane Maries Vej 30, DK 2100 Copenhagen Ø, Denmark 4 Los Alamos National Laboratory, MS D436, Los Alamos, NM 87545, U.S.A. 5 Laboratorio de astrof´ısica Espacial y F´ısica Fundamental (LAEFF), INTA, P.O. Box 50727, 28080 Madrid, Spain Received May 23; accepted August 8, 1997 Abstract. We present the catalogue of gamma-ray bursts celestial positions (the radius of the localization region is (GRB) observed with the WATCH all-sky monitor on generally smaller than 1 deg at the 3σ confidence level) board the GRANAT satellite during the period December of short-lived hard X-ray sources, which include GRBs. 1989 to September 1994. The cosmic origin of 95 bursts Another feature of the instrument relevant to observa- comprising the catalogue is confirmed either by their lo- tions of GRBs is that its detectors are sensitive over an calization with WATCH or by their detection with other X-ray energy range that reaches down to ∼ 8 keV, the do- GRB experiments. For each burst its time history and main where the properties of GRBs are known less than information on its intensity in the two energy ranges at higher energies. -
<> CRONOLOGIA DE LOS SATÉLITES ARTIFICIALES DE LA
1 SATELITES ARTIFICIALES. Capítulo 5º Subcap. 10 <> CRONOLOGIA DE LOS SATÉLITES ARTIFICIALES DE LA TIERRA. Esta es una relación cronológica de todos los lanzamientos de satélites artificiales de nuestro planeta, con independencia de su éxito o fracaso, tanto en el disparo como en órbita. Significa pues que muchos de ellos no han alcanzado el espacio y fueron destruidos. Se señala en primer lugar (a la izquierda) su nombre, seguido de la fecha del lanzamiento, el país al que pertenece el satélite (que puede ser otro distinto al que lo lanza) y el tipo de satélite; este último aspecto podría no corresponderse en exactitud dado que algunos son de finalidad múltiple. En los lanzamientos múltiples, cada satélite figura separado (salvo en los casos de fracaso, en que no llegan a separarse) pero naturalmente en la misma fecha y juntos. NO ESTÁN incluidos los llevados en vuelos tripulados, si bien se citan en el programa de satélites correspondiente y en el capítulo de “Cronología general de lanzamientos”. .SATÉLITE Fecha País Tipo SPUTNIK F1 15.05.1957 URSS Experimental o tecnológico SPUTNIK F2 21.08.1957 URSS Experimental o tecnológico SPUTNIK 01 04.10.1957 URSS Experimental o tecnológico SPUTNIK 02 03.11.1957 URSS Científico VANGUARD-1A 06.12.1957 USA Experimental o tecnológico EXPLORER 01 31.01.1958 USA Científico VANGUARD-1B 05.02.1958 USA Experimental o tecnológico EXPLORER 02 05.03.1958 USA Científico VANGUARD-1 17.03.1958 USA Experimental o tecnológico EXPLORER 03 26.03.1958 USA Científico SPUTNIK D1 27.04.1958 URSS Geodésico VANGUARD-2A